The MP and IP appear at roughly the same pulse phase from radio to \(\gamma \) -ray wavelengths, suggesting that their emission originates from a similar location in the magnetosphere at all wavebands.
Modeling of \(\gamma \) -ray light curves from the many pulsars observed by the Fermi Gamma-ray Space Telescope [1]} strongly indicates that the high-energy emission originates in the outer magnetosphere, at altitudes comparable to the light-cylinder radius [2]}, [3]}, [4]}.
Outer magnetosphere emission models, such as the outer-gap [5]}, slot-gap [6]}, and current-sheet [7]} had been proposed and studied prior to the Fermi observations, but their emission geometry seems to account for the characteristics and variety of observed \(\gamma \) -ray light curves.
In addition, Fermi has discovered a number of \(\gamma \) -ray millisecond pulsars whose radio peaks are nearly aligned with their \(\gamma \) -ray peaks [8]}, like the Crab.
Modeling both \(\gamma \) -ray and radio light curves of these pulsars with the same outer magnetosphere emission models used to model young pulsars has suggested that their radio emission may originate from very high altitudes [9]}.
Thus, in this paper we compare the phase-resolved radio polarization observations (§) that we have analyzed (§) with such models (§).
